High-resolution images of the spiral galaxy NGC 5930 have been obtained with the Planetary Camera aboard the Hubble Space Telescope in the emission lines of [O III] λλ4959, 5007 + Hβ and Hα + [N II] λλ6548, 6583, and their adjacent continua. NGC 5930 is the interacting companion of the Type 2 Seyfert galaxy NGC 5929. Five bright continuum knots, which probably represent star clusters, are found in the central ~1.5" (200 h^-1^ pc, h = H_0_/ 100 km s^-1^ Mpc^-1^) Four of these knots are associated with an elliptical ring of low-excitation gas with dimensions 2.4" x 1.6" (320 h^-1^ x 220 h^-1^ pc), while the fifth lies close to the ring's center. This gaseous ring, which probably lies in the plane of the disk, has an Hα luminosity ~7 x 10^40^ h^-2^ ergs s^-1^. Assuming that the initial mass function for 5-120 M_sun_ stars is represented by a power law with an exponent of -2.5, the Hα luminosity implies a modest star formation rate of 0.07 h^-2^ M_sun_ yr^-1^ for 5-120 M_sun_ stars, and a supernova rate from the explosion of massive stars ~3 x 10^-3^ h^- 2^ yr^-1^. This nuclear star forming region appears to be similar to other nuclear rings in spiral galaxies. It has often been argued that such nuclear rings form at or near the inner Lindblad resonance. If this is the case for NGC 5930, the small radius of the ring implies a strongly concentrated central mass distribution.