  We resolve the kinematic distance ambiguity for 266 inner Galaxy HII regions
out of a sample of 291 using existing HI and 13CO sky surveys. Our sample
contains all HII regions with measured radio recombination line (RRL) emission
over the extent of the 13CO Boston University-Five College Radio Astronomy
Observatory Galactic Ring Survey (18 deg, < l < 55 deg. and |b| < 1) and
contains ultra compact, compact, and diffuse HII regions. We use two methods
for resolving the distance ambiguity for each HII region: HI
emission/absorption (HIEA) and HI self-absorption (HISA). We find that the HIEA
and HISA methods can resolve the distance ambiguity for 72% and 87% of our
sample, respectively. When projected onto the Galactic plane, this large sample
appears to reveal aspects of Galactic structure, with spiral arm-like features
at Galactocentric radii of 4.5 and 6 kpc, and a lack of HII regions within 3.5
kpc of the Galactic center. Our HII regions are approximately in the ratio of 2
to 1 for far verses near distances. The ratio of far to near distances for
ultra-compact HII regions is 2.2 to 1. Compact HII regions are preferentially
at the near distance; their ratio of far to near distances is 1.6 to 1. Diffuse
HII regions are preferentially at the far distance; their ratio of far to near
distances is 3.8 to 1. This implies that the distinction between ultra compact
and compact HII regions is due largely to distance, and that the large angular
size of diffuse HII regions is not due solely to proximity to the Sun.
