  The evolution of star clusters in the Magellanic Clouds has been the subject
of significant recent controversy, particularly regarding the importance and
length of the earliest, largely mass-independent disruption phase (referred to
as "infant mortality"). Here, we take a fresh approach to the problem, using a
large, independent, and homogeneous data set of UBVR imaging observations, from
which we obtain the cluster age and mass distributions in both the Large and
Small Magelanic Clouds (LMC, SMC) in a self-consistent manner. We conclude that
the (optically selected) SMC star cluster population has undergone at most ~30%
(1sigma) infant mortality between the age range from about 3-10 Myr, to that of
approximately 40-160 Myr. We rule out a 90% cluster mortality rate per decade
of age (for the full age range up to 10^9 yr) at a >6sigma level. Using a
simple approach, we derive a "characteristic" cluster disruption time-scale for
the cluster population in the LMC that implies that we are observing the
INITIAL cluster mass function. Preliminary results suggest that the LMC cluster
population may be affected by <10% infant mortality.
