  Studies of Galactic HII regions are of crucial importance for studying star
formation and the evolution of the interstellar medium. Gaining an insight into
their physical characteristics contributes to a more comprehensive
understanding of these phenomena. The GLOSTAR project aims to provide a GLObal
view on STAR formation in the Milky Way by performing an unbiased and sensitive
survey. This is achieved by using the extremely wideband (4{-}8 GHz) C-band
receiver of the Karl G. Jansky Very Large Array and the Effelsberg 100 m
telescope. Using radio recombination lines observed in the GLOSTAR survey with
the VLA in D-configuration with a typical line sensitivity of 1{\sigma} {\sim}
3.0 mJy beam{^-1} at {\sim} 5 km s{^-1} and an angular resolution of 25", we
cataloged 244 individual Galactic HII regions and derived their physical
properties. We examined the mid-infrared (MIR) morphology of these HII regions
and find that a significant portion of them exhibit a bubble-like morphology in
the GLIMPSE 8 {\mu}m emission. We also searched for associations with the dust
continuum and sources of methanol maser emission, other tracers of young
stellar objects, and find that 48\% and 14\% of our HII regions, respectively,
are coextensive with those. We measured the electron temperature for a large
sample of HII regions within Galactocentric distances spanning from 1.6 to 13.1
kpc and derived the Galactic electron temperature gradient as {\sim} 372 {\pm}
28 K kpc{^-1} with an intercept of 4248 {\pm} 161 K, which is consistent with
previous studies.
