  We present structural parameters for 204 stellar clusters in the Small
Magellanic Cloud derived from fitting King and Elson, Fall, & Freeman model
profiles to the V-band surface brightness profiles as measured from the
Magellanic Clouds Photometric Survey images. Both King and EFF profiles are
satisfactory fits to the majority of the profiles although King profiles are
generally slightly superior to the softened power-law profiles of Elson, Fall,
and Freeman and provide statistically acceptable fits to ~90% of the sample. We
find no correlation between the preferred model and cluster age. The only
systematic deviation in the surface brightness profiles that we identify is a
lack of a central concentration in a subsample of clusters, which we designate
as "ring" clusters. In agreement with previous studies, we find that the
clusters in the SMC are significantly more elliptical than those in the Milky
Way. However, given the mean age difference and the rapid destruction of these
systems, the comparison between SMC and MW should not directly be interpreted
as either a difference in the initial cluster properties or their subsequent
evolution. We find that cluster ellipticity correlates with cluster mass more
strongly than with cluster age. We identify several other correlations (central
surface brightness vs. local background density, core radius vs. tidal force,
size vs. distance) that can be used to constrain models of cluster evolution in
the SMC.
