  We report on an observation of SGR 1627-41 made with the Chandra X-ray
Observatory on 2011 June 16. Approximately three years after its outburst
activity in 2008, the source's flux has been declining, as it approaches its
quiescent state. For an assumed power-law spectrum, we find that the absorbed
2--10 keV flux for the source is $1.0^{+0.3}_{-0.2} \times 10^{-13} erg cm^{-2}
s^{-1}$ with a photon index of $2.9 \pm 0.8$ ($N_H=1.0\times10^{23}$ cm^{-2}).
This flux is approximately consistent with that measured at the same time after
the source's outburst in 1998. With measurements spanning 3 years after the
2008 outburst, we analyze the long-term flux and spectral evolution of the
source. The flux evolution is well described by a double exponential with decay
times of 0.5 $\pm$ 0.1 and 59 $\pm$ 6 days, and a thermal cooling model fit
suggests that SGR 1627-41 may have a hot core ($T_c ~ 2\times 10^8$ K). We find
no clear correlation between flux and spectral hardness as found in other
magnetars. We consider the quiescent X-ray luminosities of magnetars and the
subset of rotation-powered pulsars with high magnetic fields ($B >~ 10^{13}$ G)
in relation to their spin-inferred surface magnetic-field strength, and find a
possible trend between the two quantities.
