  We present UV (2300 Ang) images, obtained with the HST Faint Object Camera,
of the central 20'' of five galaxies containing circumnuclear star-forming
rings. The five galaxies are from a well-defined sample of 103 normal, nearby
galaxies we have observed with HST. At the HST resolution (0.05''), the rings
break up into discrete star-forming clumps, each composed of many luminous and
compact ($R \ltorder 5$ pc) star clusters. These objects are similar to those
that have been recently reported in colliding and starburst galaxies, and in
several other circumnuclear rings. A large fraction, 15%--50%, of the UV
emission originates in these compact clusters. Compact clusters therefore may
be the preferred mode of star formation in starburst environments. For one
galaxy, NGC 2997, we measure the UV-optical colors of the individual clusters
using an archival HST WFPC2 image at 6000 Ang . Comparing the colors and
luminosities to starburst population synthesis models, we show that the
clusters are less than 100 Myr old and have masses of at least a few $10^3
M_{\odot}$, with some as high as $10^5 M_{\odot}$. The UV extinction to those
clusters that are detected in the UV is at most a factor of 10. In NGC 2997,
the limits on the masses and the ages of the young clusters indicate that these
objects will remain bound and evolve into globular clusters. The luminosity
function of the clusters in the rings is similar in shape to those measured for
super star clusters in other star-forming galaxies, and extends to luminosities
lower by several orders of magnitude. All five of the UV-detected circumnuclear
rings occur in barred or weakly barred spiral galaxies of type Sc or earlier.
None of the five rings has an active nucleus at its center, arguing against a
direct correspondence between circumnuclear star formation and nuclear
