  We present B, V, R, and H alpha photometry of 8 clusters in the Small
Magellanic Cloud, 5 in the Large Magellanic Cloud, and 3 Galactic clusters, and
use 2 color diagrams (2-CDs) to identify candidate Be star populations in these
clusters. We find evidence that the Be phenomenon is enhanced in low
metallicity environments, based on the observed fractional early-type candidate
Be star content of clusters of age 10-25 Myr. Numerous candidate Be stars of
spectral types B0 to B5 were identified in clusters of age 5-8 Myr, challenging
the suggestion of Fabregat & Torrejon (2000) that classical Be stars should
only be found in clusters at least 10 Myr old. These results suggest that a
significant number of B-type stars must emerge onto the zero-age-main-sequence
as rapid rotators. We also detect an enhancement in the fractional content of
early-type candidate Be stars in clusters of age 10-25 Myr, suggesting that the
Be phenomenon does become more prevalent with evolutionary age. We briefly
discuss the mechanisms which might contribute to such an evolutionary effect. A
discussion of the limitations of utilizing the 2-CD technique to investigate
the role evolutionary age and/or metallicity play in the development of the Be
phenomenon is offered, and we provide evidence that other B-type objects of
very different nature, such as candidate Herbig Ae/Be stars may contaminate the
claimed detections of ``Be stars'' via 2-CDs.
