  We have studied the supernova remnant G67.7+1.8 with the Chandra X-ray
observatory. The remnant's X-ray morphology correlates well with the double-arc
structure seen at radio wavelength. The X-ray spectra of the northern and
southern rim of G67.7+1.8 exhibit emission line features of highly ionized
metals, which suggests that most of the observed X-rays originate in a thermal
plasma. We find magnesium, silicon, and sulphur are overabundant relative to
the solar values. Gaussian emission lines at $\sim4$ keV and $\sim7$ keV are
detected. The $\sim4$ keV line is consistent with K-emission lines from
$^{44}$Ca and/or $^{44}$Sc whereas the $\sim7$ keV line feature may arise from
unresolved Fe-K lines. Chandra's sub-arcsecond angular resolution allowed us to
detect four faint point sources located within $\sim1.5$ arc-minutes of the
geometrical remnant center. Among these objects, CXOU195424.75+312824.9 and
CXOU195429.82+312834.1 do not have optical counterparts, leaving them as
candidates for a possible compact stellar remnant.
