  We analyse a Chandra observation of the rich globular cluster NGC 362,
finding 33 X-ray sources within 1' (1.2 half-mass radii) of the cluster center.
Spectral analysis of the brightest source (X1) shows blackbody-like emission,
indicating it is likely a quiescent low-mass X-ray binary; we find a possible
counterpart that falls in the sub-subgiant region. We use HST UV Globular
Cluster Survey (HUGS) photometry to identify 15 potential optical/UV
counterparts to these X-ray sources, including two background AGN. We identify
no likely CVs, probably due to crowding in optical filters in the core, though
we predict of order 8 CVs among the detected X-ray sources. We identify three
other sub-subgiants and two red straggler counterparts, which are likely
powered by coronal activity, along with five other potential coronally active
binary counterparts to three X-ray sources. Finally, we note two unusual
counterpart candidates that lie to the red of the red giant branch in V_606 -
I_814, and shift well to the blue of the red giant branch in ultraviolet
colour-magnitude diagrams. These systems seem to contain a red giant with a
distorted evolutionary history, plus a bright blue light source, either a blue
straggler star (an Algol-like system) or an accreting white dwarf (a
long-period CV, or a symbiotic star).
