  We have observed the massive star forming region, IRAS 18507+0121, at
millimeter wavelengths in 3 mm continuum emission and H13CO+(J=1-0) and
SiO(v=0, J=2-1) line emission, and at near-infrared wavelengths between 1.2 and
2.1 microns. Two compact molecular cores are detected: one north and one south
separated by about 40". The northern molecular core contains a newly
discovered, deeply embedded, B2 protostar surrounded by several hundred solar
masses of warm gas and dust, G34.4+0.23 MM. Based on the presence of warm dust
emission and the lack of detection at near-infrared wavelengths, we suggest
that G34.4+0.23 MM may represent the relatively rare discovery of a massive
protostar (e.g. analogous to a low-mass "Class 0" protostar). The southern
molecular core is associated with a near-infrared cluster of young stars and an
ultracompact (UC) HII region, G34.4+0.23, with a central B0.5 star. The
fraction of near-infrared stars with excess infrared emission indicative of
circumstellar material is greater than 50% which suggests an upper limit on the
age of the IRAS 18507+0121 star forming region of 3 Myrs.
