  We characterize the stellar population of the poorly explored young stellar
cluster NGC 3293 at the northwestern periphery of the Carina Nebula Complex, in
order to evaluate the cluster age and the mass function, and to test claims of
an abnormal IMF and a deficit of M <= 2.5 M_sun stars. We performed a deep (70
ksec) X-ray observation of NGC 3293 with Chandra and detected 1026 individual
X-ray point sources. We identify counterparts for 74% of the X-ray sources in
deep near-infrared images. Our data clearly show that NGC 3293 hosts a large
population of solar-mass stars, refuting claims of a lack of M <= 2.5 M_sun
stars. The analysis of the color magnitude diagram suggests an age of ~8-10 Myr
for the low-mass population of the cluster. There are at least 511 X-ray
detected stars with color magnitude positions that are consistent with young
stellar members within 7 arcmin of the cluster center. The number ratio of
X-ray detected stars in the 1-2 M_sun range versus the M >= 5 M_sun stars
(known from optical spectroscopy) is consistent with the expectation from a
normal field initial mass function. Most of the early B-type stars and 20% of
the later B-type stars are detected as X-ray sources. Our data shows that NGC
3293 is one of the most populous stellar clusters in the entire Carina Nebula
Complex. The cluster probably harbored several O-type stars, whose supernova
explosions may have had an important impact on the early evolution of the
Carina Nebula Complex.
