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The Bolocam Galactic Plane Survey (BGPS) data for a six square degree regionof the Galactic plane containing the Galactic center is analyzed and comparedto infrared and radio continuum data. The BGPS 1.1 mm emission consists ofclumps interconnected by a network of fainter filaments surrounding cavities, afew of which are filled with diffuse near-IR emission indicating the presenceof warm dust or with radio continuum characteristic of HII regions or supernovaremnants. New 350 {\mu}m images of the environments of the two brightestregions, Sgr A and B, are presented. Sgr B2 is the brightest mm-emitting clumpin the Central Molecular Zone and may be forming the closest analog to a superstar cluster in the Galaxy. The Central Molecular Zone (CMZ) contains thehighest concentration of mm and sub-mm emitting dense clumps in the Galaxy.Most 1.1 mm features at positive longitudes are seen in silhouette against the3.6 to 24 {\mu}m background observed by the Spitzer Space Telescope. However,only a few clumps at negative longitudes are seen in absorption, confirming thehypothesis that positive longitude clumps in the CMZ tend to be on thenear-side of the Galactic center, consistent with the suspected orientation ofthe central bar in our Galaxy. Some 1.1 mm cloud surfaces are seen in emissionat 8 {\mu}m, presumably due to polycyclic aromatic hydrocarbons (PAHs). A~0.2\degree (~30 pc) diameter cavity and infrared bubble between l \approx0.0\degree and 0.2\degree surrounds the Arches and Quintuplet clusters and SgrA. The bubble contains several clumpy dust filaments that point toward SgrA\ast; its potential role in their formation is explored. [abstract truncated]

The Bolocam Galactic Plane Survey IV: 1.1 and 0.35 mm Dust Continuum Emission in the Galactic Center Region