  We present results from a 34 ks Chandra/ACIS-S observation of the nearby
(d=3.1 Mpc) lenticular galaxy NGC 5102, previously shown to have an unusually
low X-ray luminosity. We detect eleven X-ray point sources within the the
$D_{25}$ optical boundary of the galaxy (93% of the light), one third to one
half of which are likely to be background AGN. One source is coincident with
the optical nucleus and may be a low-luminosity AGN. Only two sources with an
X-ray luminosity greater than 10$^{37}$ ergs s$^{-1}$ in the 0.5-5.0 keV band
were detected, one of which is statistically likely to be a background AGN. We
expected to detect 6 such luminous sources if the XRB population scales
linearly with optical magnitude of the host galaxy. NGC 5102 has an unusually
low number of XRBs. NGC 5102 is unusually blue for its morphological type, and
has undergone at least two recent bursts of star formation. We present the
results of optical/UV spectral synthesis analysis and demonstrate that a
significant fraction ($>$50%) of the stars in this galaxy are comparatively
young ($<3\times10^9$ years old). If the lack of X-ray binaries is related to
the relative youth of most of the stars, this would support models of LMXB
formation and evolution that require wide binaries to shed angular momentum on
a timescale of Gyrs. We find that NGC 5102 has an unusually low specific
frequency of globular clusters ($S_N\sim$0.4), which could also explain the
lack of LMXBs. We also detect diffuse X-ray emission in the central $\sim$1 kpc
of the galaxy. This hot gas is most likely a superbubble created by multiple
supernovae of massive stars born during the most recent star burst, and is
driving the shock into the ISM which was inferred from optical observations.
