  We discuss the present state of knowledge and thought concerning the spread
in age found among Galactic globular clusters, with some discussion of the
implications for what happened during the earliest stages of the formation of
the Milky Way Galaxy. Differential observational techniques to derive the
relative age differences among clusters of similar metallicity are discussed in
detail. We conclude that as of the current date (mid-April 1996) the state of
the field is still somewhat muddled. However, we believe that there is now a
substantial body of evidence --- including a particularly revealing
intercomparison of the color-magnitude diagrams of \ngc{1851}, \ngc{288}, and
\ngc{362} presented here --- indicating that age is {\it not\/} the dominant
second parameter determining the shape of globular clusters' horizontal
branches. If our assertion is correct, then apart from a handful of anomalous
clusters that may well have been captured from a satellite dwarf galaxy, there
is no strong evidence either for a significant spread in age among clusters of
a given metal abundance or for a systematic variation of mean age with
Galactocentric distance. On the question of whether there is a significant age
difference between metal-poor and metal-rich clusters, we feel compelled to
fall back on the Scottish verdict: ``Unproven.'' Data now being collected by
numerous groups in various subdisciplines may resolve the remaining controversy
within a few years.
