Abstract We observed CO $J =$ 1-0 and HCN $J =$ 1-0 line emission toward a high-velocity, compact molecular cloud, CO0.02-0.02, near the center of our Galaxy, using the Nobeyama Millimeter Array (NMA). A CO velocity-integrated map with a resolution of 4.3”$\times$2.4” shows two oval clumps with sizes of 0.8pc. These clumps are seperated by 1.2pc, being located at the eastern and southwestern peripheries of the CO0.02-0.02 cloud. The overall distribution of HCN emission coincides with that taken with the Nobeyama 45m telescope. The HCN velocity-integrated map with a resolution of 6.1”$\times$3.4” shows two prominent peaks in the cloud center. Both NMA maps at $V_{\rm LSR}$$\sim$110kms$^{-1}$ show an arc-shaped edge in the southeast, which may correspond to the edge of the “emission cavity” found in the CO $J =$ 3-2 integrated-intesity map. We also noticed a faint radio continuum “arc” that encircles the bulk of the CO0.02-0.02 cloud. These results support the notion that CO0.02-0.02 has been accelerated, heated, and compressed in a series of supernova shocks that occurred within the last (3-5)$\times$10$^{4}$yr. We suggest that a massive compact cluster with an age of 10-30Myr is responsible for the formation of the CO0.02-0.02 cloud.