  We present the age distributions for star clusters and individual stars in
the Small Magellanic Cloud (SMC) based on data from the Magellanic Clouds
Photometric Survey by Zaritsky and collaborators. The age distribution of the
SMC clusters shows a steep decline, dN_{cluster}/dt \propto t^{-0.85\pm0.15},
over the period 10^7 < t <10^9 yr. This decline is essentially identical to
that observed previously for more massive clusters in the merging Antennae
galaxies, and also for lower-mass embedded clusters in the solar neighborhood.
The SMC cluster age distribution therefore provides additional evidence for the
rapid disruption of star clusters (``infant mortality''). These disrupted
clusters deliver their stars to the general field population, implying that the
field star age distribution, dN_{fld star}/dt, should have an inverse relation
to dN_{cluster}/dt if most stars form initially in clusters. We make specific
predictions for dN_{fldstar}/dt based on our cluster disruption models, and
compare them with current data available for stars in the SMC. While these data
do not extend to sufficiently young ages for a definitive test, they are
consistent with a scenario wherein most SMC stars formed in clusters. Future
analyses of dN_{fldstar}/dt that extend down to ages of approximately few
million years are needed to verify the age relationship between stars residing
in clusters and in the field.
