ABSTRACT: The scattering diameters of Sgr A^* and several nearby OH masers (~ 1'' at 1 GHz) indicate that a region of enhanced scattering is along the line of sight to the Galactic center (GC). We first demonstrate that the enhanced scattering region is likely to be associated with the GC; a likelihood analysis indicates that the GC-scattering region separation is DELTA _\mathrmGC = 150 pc. The extent of the region in Galactic longitude is \psi l = 0.\!\!^o5-1^o. At the distance of the GC, D_\mathrmGC, the equivalent linear size of the scattering region, \psi l D_\mathrmGC, is comparable to DELTA _\mathrmGC. The close correspondence between DELTA _\mathrmGC and \psi l D_\mathrmGC suggests that the scattering region encloses the Galactic center. The strength of scattering is not uniform across the region, however, and order of magnitude changes in the strength of scattering are seen over scales of a few arcminutes (10-20 pc at the distance of the GC). A scattering region that is clumpy on scales of 10-20 pc, with an angular extent of 0.\!\!^o5-1^o, leads us to favor an ``interface'' model, in which the scattering arises on the ionized surfaces of molecular clouds exposed to the X-ray emitting, 107 K gas; in this model the scattering medium is hot (Te ~ 106 K) and dense (n_\mathrme ~ 10 cm-3). We also illustrate the impact of the scattering region on the search for pulsars in the Galactic center. We stress the uniqueness of the GC scattering region, probably resulting from the high-pressure environment in the GC.