  In this paper we have examined the internal dynamics of the globular cluster
NGC 362. A V band surface brightness profile (SBP) was constructed from CCD
images, and, after it was determined that the cluster is not post
core-collapse, fit with single- and multi-mass King-Michie (KM) models. The
total cluster luminosity is 1.70 $\pm 0.1 \times 10^5$ L$_V$\sol. A total of
285 stellar spectra were obtained of 215 stars for radial velocity
determinations. Four stars showed strong evidence for radial velocity
variations and are probably members of binary systems. The true cluster binary
fraction was determined from simulations to be 0.15 for circular orbits or 0.27
for orbits with a distribution function $f(e) = e$ ($e$ is eccentricity). This
relatively high binary detection frequency may indicate that NGC 362 is
overabundant in binaries compared to other clusters. The 208 remaining stars
showed no sign of rotation. The best agreement with both the kinematic data and
the SBP were for shallow mass functions $x = 0.0 - 0.5$ and intermediate
amounts of anisotropy in the velocity dispersion tensor. The cluster mass is M
= $2.5 - 3.5 \times 10^5$ M\sol\ for a global mass-to-light ratio of M/L$_V$ =
1.5 - 2.0 M\sol/L$_V$\sol. This low value for $x$ is in disagreement with the
correlation between $x$ and the height above the Galactic disk seen for a
sample of other clusters. The results are also different from the sharp turn-up
in the low mass end of mass functions derived from some deep luminosity
functions of three other globular clusters.
