  Wide field images obtained with WIRCam and MegaCam on the
Canada-France-Hawaii Telescope are used to probe the spatial distribution of
young stars in the Sc galaxy NGC 2403. Bright main sequence stars and blue
supergiants are detected out to projected galactocentric distances of ~14 kpc
(~7 disk scale lengths) along the major axis. The star formation rate (SFR) in
the disk of NGC 2403 during the past 10 Myr has been 1 solar masses per year
based on the number of bright main sequence stars. The radially-averaged number
density of red supergiants (RSGs) per unit r-band surface brightness is
constant throughout the disk, indicating that (1) RSGs follow the integrated
r-band light, and (2) the SFR per unit mass has been constant with radius when
averaged over time scales of a few tens of millions of years. The mean color of
RSGs varies with galactocentric distance, suggesting that there is a
metallicity gradient among recently formed stars. A comparison of the
radially-averaged number density of bright main sequence stars also indicates
that the SFR per unit stellar mass in NGC 2403 has been ~3 times higher than in
NGC 247 during recent epochs, and this is in rough agreement with what would be
predicted from the far infrared fluxes of these galaxies. Finally, the data are
used to investigate the extraplanar regions of NGC 2403. A population of M
giants with peak brightness M_K = -8 is detected at projected distances between
12 and 14 kpc above the disk plane, and six new globular cluster candidates are
identified.
