  We analyze the galaxy population and dynamics of the galaxy cluster Abell 576
using 281 redshifts (230 new), R band CCD galaxy photometry over a 2h^{-1} Mpc
by 2h^{-1} Mpc region centered on the cluster, an Einstein IPC image, and an
Einstein MPC spectrum. The cluster galaxies with emission lines in their
spectra have a larger velocity dispersion and are significantly less clustered
on this 2h^{-1} Mpc scale than galaxies without emission lines. We show that
excluding the emission line galaxies decreases the velocity dispersion by 18%
and the virial mass estimate by a factor of two. The central cluster region
contains a non--emission galaxy population and an intracluster medium which are
significantly cooler (sigma_{core}=387^{+250}_{-105}~km/s and
T_X=1.6^{+0.4}_{-0.3}~keV at 90\% confidence) than the global populations
(sigma=977^{+124}_{-96}~km/s for the non--emission population and T_X>4~keV at
90% confidence). Because (1) the low dispersion population is no more luminous
than the global population and (2) the evidence for a cooling flow is weak, we
suggest that the cluster core may contain the remnants of a lower mass
subcluster. We examine the cluster mass, baryon fraction and luminosity
function. The cluster virial mass varies significantly depending on the galaxy
sample used. Consistency between the hydrostatic and virial estimators can be
achieved if (1) the gas temperature at r\sim1h^{-1}~Mpc is T_X\sim8keV (the
best fit value) and (2) several velocity outliers are excluded from the virial
calculation. Although the best fit Schechter function parameters and the ratio
of galaxy to gas mass are typical of other clusters, the baryon fraction is
relatively low. Using a lower limit to the binding mass, we show that the gas
mass fraction is \le3h^{-3/2}% and the baryon fraction is \le6%.
