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. Differnetial 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 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 my 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 idfference tween 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 subsdisciplines may resolve the remaining controversy within a few years.