  New optical HST, Spitzer, GALEX, and Chandra observations of the
single-nucleus, luminous infrared galaxy (LIRG) merger IC 883 are presented.
The galaxy is a member of the Great Observatories All-sky LIRG Survey (GOALS),
and is of particular interest for a detailed examination of a luminous
late-stage merger due to the richness of the optically-visible star clusters
and the extended nature of the nuclear X-ray, mid-IR, CO and radio emission. In
the HST ACS images, the galaxy is shown to contain 156 optically visible star
clusters distributed throughout the nuclear regions and tidal tails of the
merger, with a majority of visible clusters residing in an arc ~ 3-7 kpc from
the position of the mid-infrared core of the galaxy. The luminosity functions
of the clusters have an alpha_F435W ~ -2.17+/-0.22 and alpha_F814W ~
-2.01+/-0.21. Further, the colors and absolute magnitudes of the majority of
the clusters are consistent with instantaneous burst population synthesis model
ages in the range of a few x10^7 - 10^8 yrs (for 10^5 M_sun clusters), but may
be as low as few x10^6 yrs with extinction factored in. The X-ray and mid-IR
spectroscopy are indicative of predominantly starburst-produced nuclear
emission, and the star formation rate is ~ 80 M_sun / yr. The kinematics of the
CO emission and the morphology of both the CO and radio emission are consistent
with the nuclear starburst being situated in a highly inclined disk 2 kpc in
diameter with an infrared surface brightness mu_IR ~ 2x10^11 L_sun kpc^-2, a
factor of 10 less than that of the Orion star-forming region. Finally, the
detection of the [Ne V] 14.32 um emission line is evidence that an AGN is
present. The faintness of the line (i.e., [Ne V] / [Ne II] um ~ 0.01) and the
small equivalent width of the 6.2 um PAH feature ($= 0.39\mu$m) are both
indicative of a relatively weak AGN. (abridged)
