  We present the spatially-resolved star formation and chemical enrichment
history of the Small Magellanic Cloud (SMC) across the entire central $4-degree
x 4.5-degree area of the main body, based on UBVI photometry from our
Magellanic Clouds Photometric Survey. We find that 1) approximately 50% of the
stars that ever formed in the SMC formed prior to 8.4 Gyr ago (z >1.2 for WMAP
cosmology), 2) the SMC formed relatively few stars between 8.4 and 3 Gyr ago,
3) there was a rise in the mean star formation rate during the most recent 3
Gyr punctuated by "bursts" at ages of 2.5, 0.4, and 0.06 Gyr, 4) the bursts at
2.5 and 0.4 Gyr are temporally coincident with past perigalactic passages of
the SMC with the Milky Way, 5) there is preliminary evidence for a large-scale
annular structure in the 2.5 Gyr burst, and 6) the chemical enrichment history
derived from our analysis is in agreement with the age-metallicity relation of
the SMC's star clusters. Consistent interpretation of the data required an ad
hoc correction of 0.1-0.2 mag to the B-V colors of 25% of the stars; the cause
of this anomaly is unknown, but we show that it does not strongly influence our
results.
