  The Galactic Bulge has long been assumed to be a largely old stellar
population. However, some recent studies based on observations with the HST
WF/PC-1 and WFPC2 of stars in the Galactic Bulge have concluded that the old
population may not make up more then 30% of the total. Other studies using
HST/WFPC2 differential studies of `Bulge' globular clusters and field stars
have found the bulge to be comparable in age to the Galactic Halo. A
complication in all these studies is the presence of a substantial population
of stars which mimic a young bulge population, but which may be, and are often
assumed to be, foreground disk stars whose reddening and distance distributions
happen to mimic a young bulge turnoff. We show, using number counts in
HST/WFPC2 colour-magnitude diagrams of both field stars in the Bulge and of two
`bulge' and one `disk' globular cluster (NGC6528, NGC6553, and NGC5927) that
the stars interpreted as young in fact are foreground disk stars. Thus, we
confirm that the bulk of the bulge field stars in Baade's Window are old. The
existence of a young metal-rich population cannot, however, be ruled out from
our data. We also test for age and metallicity gradients using the CMD of a
metal-rich globular cluster as an empirical isochrone and derive a metallicity
difference of <0.2 dex between Baade's window and SGR-I window.
