A large scale configuration-interaction (CI) calculation is performed of excitation energies for 109 fine-structure levels belonging to the configurations (1s22s22p6)3s23p(2Po), 3s3p2(2S, 2P, 2D, 4P), 3s2 3d(2D), 3p3(4So, 2Po, 2Do), 3s3p(3Po) 3d(2Po, 2Do, 2Fo, 4Po, 4Do, 4Fo), 3s3p(1Po)3d(2Po, 2Do, 2Fo), 3p2(1S)3d(2D), 3p2(1D)3d(2S, 2P, 2D), 3p2(3P)3d(2P, 2D, 4P), 3s3d2(2S, 2P, 2D, 4P), 3p3d2(1S)(2Po), 3p3d2(1D)(2Po, 2Do, 2Fo), 3p3d2(1G)(2Fo), 3p3d2(3P)(2Po, 2Do, 4So, 4Po, 4Do), 3p3d2(3F)(2Do, 2Fo, 4Do, 4Fo), 3s24s(2S), 3s24p(2Po), 3s24d(2D), 3s24f(2Fo), 3s3p(3Po)4s(2Po, 4Po), and 3s3p(1Po)4s(2Po) of Al-like Titanium, using the CIV3 computer code of Hibbert. The states are represented by very extensive CI wave functions. The relativistic effects in intermediate coupling are incorporated by means of the Breit–Pauli Hamiltonian, which consists of the non-relativistic term plus the one-body mass correction, Darwin term, and spin-orbit, spin-other-orbit, and spin-spin operators. The errors, which often occur with sophisticated ab initio atomic structure calculations, are reduced to a manageable magnitude by adjusting the diagonal elements of the Hamiltonian matrices. Our calculated excitation energies, including their ordering, are in excellent agreement with the available experimental results. We predict new data for several levels where no other theoretical and experimental results are available. The mixing among several fine-structure levels is found to be very strong, with most of the strongly mixed levels belonging to the (1s22s22p6)3p23d and 3p3d2 configurations. The enormous mixing among several fine-structure levels makes it very difficult to identify them correctly. Perhaps, that may be the reason for the lack of experimental results for these levels. We believe that our extensive calculated values can guide experimentalists identify the fine-structure levels. From our radiative decay rates, we have calculated radiative lifetimes of the high angular momentum and high spin levels 3s3p3d(4FJ). The large difference in the lifetime of the 3s3p3d(4Fo1.5) level obtained from our two calculations (ab initio & adjusted energies) is explained. We conclude by recommending remeasurements of the energy levels of the 3s3p3d(4Fo1.5) in Ti X and Fe XIV to reduce the current large experimental uncertainties.