  We present stellar age distributions of the Milky Way (MW) bulge region using
ages for $\sim$6,000 high-luminosity ($\log(g) < 2.0$), metal-rich ($\rm [Fe/H]
\ge -0.5$) bulge stars observed by the Apache Point Observatory Galactic
Evolution Experiment (APOGEE). Ages are derived using {\it The Cannon}
label-transfer method, trained on a sample of nearby luminous giants with
precise parallaxes for which we obtain ages using a Bayesian isochrone-matching
technique. We find that the metal-rich bulge is predominantly composed of old
stars ($>$8 Gyr). We find evidence that the planar region of the bulge
($|Z_{\rm GC}| \le 0.25$ kpc) enriched in metallicity, $Z$, at a faster rate
($dZ/dt \sim$ 0.0034 ${\rm Gyr^{-1}}$) than regions farther from the plane
($dZ/dt \sim$ 0.0013 ${\rm Gyr^{-1}}$ at $|Z_{\rm GC}| > 1.00$ kpc). We
identify a non-negligible fraction of younger stars (age $\sim$ 2--5 Gyr) at
metallicities of $\rm +0.2 < [Fe/H] < +0.4$. These stars are preferentially
found in the plane ($|Z_{\rm GC}| \le 0.25$ kpc) and between $R_{\rm cy}
\approx 2-3$ kpc, with kinematics that are more consistent with rotation than
are the kinematics of older stars at the same metallicities. We do not measure
a significant age difference between stars found in and outside of the bar.
These findings show that the bulge experienced an initial starburst that was
more intense close to the plane than far from the plane. Then, star formation
continued at super-solar metallicities in a thin disk at 2 kpc $\lesssim R_{\rm
cy} \lesssim$ 3 kpc until $\sim$2 Gyr ago.
