The first evidence for nonthermal broadening of X-ray lines in a quiescent active region was based on a single observation of a limb active region by the Flat Crystal Spectrometer (FCS) on the Solar Maximum Mission (SMM) satellite /1/. With the renewal of SMM operations, the FCS has been used to further investigate this phenomenon. On 28 April 1984, a map of Mg XI resonance line profiles was made for a bright area in NOAA Active Region 4474 during a nonflaring period. The narrowest line profiles are consistent with the nominal instrumental width plus a thermal width equivalent to about 3 × 106 K, the temperature derived from line ratios of O VIII, Ne IX, and Mg XI. The broadest line profiles are consistent with the instrumental width plus a thermal width equivalent to about 7 × 106 K, but a substantial amount of plasma at this temperature would result in much greater flux in the FCS higher-temperature channels than was seen. If the excess width is attributed solely to plasma turbulence, the corresponding velocity would be about 40+/-10 km s-1. If associated with energy dissipation, such turbulent motions could have important consequences for coronal heating. Correlations of line widths and intensities with magnetic and Hα structures are investigated.