  We present HST photometry and Keck spectroscopy of globular clusters (GCs) in
the nearby S0 galaxy NGC 7457. The V-I color-magnitude diagram of GCs lacks the
clear bimodality present in most early-type galaxies; there may be a
significant population of intermediate-color objects. Of 13
spectroscopically-observed GCs, two are unusually metal-rich and feature bright
[O III] emission lines. We conclude that one probably hosts a planetary nebula
and the other a supernova remnant. Such emission line objects should be more
common in an intermediate-age stellar population than in an old one. We
therefore suggest that, in addition to the typical old metal-rich and old
metal-poor GC subpopulations, there may be a third subpopulation of
intermediate age. Such a subpopulation may have been formed ~2-3 Gyr ago, in
the same star-forming event that dominates the stellar population of the center
of the galaxy.
