  1WGA J1346.5-6255 is a ROSAT X-ray source found within the radio lobes of the
supernova remnant (SNR) G309.2-00.6. This source also appears to coincide with
the bright and early-type star HD 119682, which is in the middle of the
galactic open cluster NGC 5281. The radio morphology of the remnant, consisting
of two brightened and distorted arcs of emission on opposite sides of the 1WGA
J1346.5-6255 source and of a jet-like feature and break in the shell, led to
the suggestion that 1WGA J1346.5-6255/G309.2-00.6 is a young analog of the
microquasar SS 433 powering the W50 nebula. This motivated us to study this
source at X-ray and optical wavelengths. We here present new Chandra
observations of 1WGA J1346.5-6255, archival XMM-Newton observations of
G309.2-00.6, and optical spectroscopic observations of HD 119682, in order to
search for X-ray jets from 1WGA J1346.5-6255, study its association with the
SNR, and test for whether HD 119682 represents its optical counterpart. We do
not find evidence for jets from 1WGA J1346.5-6255 down to an unabsorbed flux of
2.6E-13 ergs/cm2/s (0.5-7.5 keV), we rule out its association with G309.2-00.6,
and we confirm that HD 119682 is its optical counterpart. We derive a distance
of 1.2+/-0.3 kpc, which is consistent with the distance estimate to NGC 5281
(1.3+/-0.3 kpc), and much smaller than the distance derived to the SNR
G309.2-00.6. We discuss the nature of the source, unveil that HD 119682 is a Be
star and suggest it is a new member of the recently proposed group of
$\gamma$-Cas analogs. The Chandra and XMM X-ray lightcurves show variability on
timescales of hundreds of seconds, and the presence of a possible period of
about 1500 s that could be the rotational period of an accreting neutron star
or white dwarf in this $\gamma$-Cas analog.
