ABSTRACT We present optical and near-infrared (NIR) light curves and optical spectra of SN 2013dx, associated with the nearby (redshift 0.145) gamma-ray burst GRB 130702A. The prompt isotropic gamma-ray energy released from GRB 130702A is measured to be E γ , iso = 6.4 − 1.0 + 1.3 × 10 50 ?> erg (1 keV to 10 MeV in the rest frame), placing it intermediate between low-luminosity GRBs like GRB 980425/SN 1998bw and the broader cosmological population. We compare the observed g ′ r ′ i ′ z ′ ?> light curves of SN 2013dx to a SN 1998bw template, finding that SN 2013dx evolves ∼20% faster (steeper rise time), with a comparable peak luminosity. Spectroscopically, SN 2013dx resembles other broad-lined SNe Ic, both associated with (SN 2006aj and SN 1998bw) and lacking (SN 1997ef, SN 2007I, and SN 2010ah) gamma-ray emission, with photospheric velocities around peak of ∼ 21,000 km s−1. We construct a quasi-bolometric ( g ′ r ′ i ′ z ′ yJ ?> ) light curve for SN 2013dx, only the fifth GRB-associated SN with extensive NIR coverage and the third with a bolometric light curve extending beyond Δ t > 40 days ?> . Together with the measured photospheric velocity, we derive basic explosion parameters using simple analytic models. We infer a 56Ni mass of M Ni = 0.37 ± 0.01 ?> M ⊙ ?> , an ejecta mass of M ej = 3.1 ± 0.1 ?> M ⊙ ?> , and a kinetic energy of E K = ( 8.2 ± 0.43 ) × 10 51 ?> erg (statistical uncertainties only), consistent with previous GRB-associated supernovae. When considering the ensemble population of GRB-associated supernovae, we find no correlation between the mass of synthesized 56Ni and high-energy properties, despite clear predictions from numerical simulations that M Ni ?> should correlate with the degree of asymmetry. On the other hand, M Ni ?> clearly correlates with the kinetic energy of the supernova ejecta across a wide range of core-collapse events.