  The WFPC2 of the HST has been used to obtain high-resolution images of NGC
4038/4039 that go roughly 3 magnitudes deeper in V than previous observations
made during Cycle 2 (-14 < M_V < -6). To first order the luminosity function
(LF) is a power law, with exponent \alpha = -2.12 +/- 0.04. However, after
decoupling the cluster and stellar LFs, which overlap in the range -9 < M_V <
-6, we find an apparent bend in the young cluster LF at approximately M_V =
-10.4. The LF has a power law exponent -2.6 +/- 0.2 in the brightward and -1.7
+/- 0.2 in the faintward. The bend corresponds to a mass ~ 10^5 M_{\odot}, only
slightly lower than the characteristic mass of globular clusters in the Milky
Way (~2x10^5 M_{\odot}). The star clusters of the Antennae appear slightly
resolved, with median effective radii of 4 +/- 1 pc, similar to or perhaps
slightly larger than those of globular clusters in our Galaxy. However, the
radial extents of some of the very young clusters (ages < 10 Myr) are much
larger than those of old globular clusters. A combination of the UBVI colors,
\Halpha morphology, and GHRS spectra enables us to age-date the clusters in
different regions of The Antennae. We find two groups of young star clusters
with ages <~ 20Myr and ~100Myr, as well as an intermediate-age group (~500 Myr)
and a handful of old globular clusters from the progenitor galaxies. Age
estimates derived from GHRS spectroscopy yield 3 +/- 1 Myr for Knot K (just
south of the nucleus of NGC 4038) and 7 +/- 1 Myr for Knot S in the Western
Loop, in good agreement with ages derived from the UBVI colors. Effective
gas-outflow velocities from Knots S and K are estimated to be about 25-30 km/s.
However, the measured widths of the interstellar absorption lines suggest
dispersion velocities of ~400 km/s along the lines of sight to Knots S and K.
