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We present a study of signatures of on-going star formation in a sample ofprotostellar objects with enhanced 4.5 {\mu}m emission ('green' sources) nearthe Galactic center. To understand how star formation in the Galactic centerregion compares to that of the Galactic disk, we used the Expanded Very LargeArray to observe radiatively excited Class II 6.7 GHz CH3OH masers andcollisionally excited Class I 44 GHz CH3OH masers, both tracers of high-massstar formation, toward a sample of 34 Galactic center and foreground 'green'sources. We find that 33\pm15% of Galactic center sources are coincident with6.7 GHz masers, and that 44\pm17% of foreground sources are coincident with 6.7GHz masers. For 44 GHz masers, we find correlation rates of 27\pm13% and25\pm13% for Galactic center green sources and foreground green sources,espectively. Based on these CH3OH maser detection rates, as well ascorrelations of green sources with other tracers of star formation, such as 24{\mu}m emission and infrared dark clouds (IRDCs), we find no significantdifference between the green sources in the Galactic center and thoseforeground to it. This suggests that once the star formation process has begun,the environmental differences between the Galactic center region and theGalactic disk have little effect on its observational signatures. We do find,however, some evidence that may support a recent episode of star formation inthe Galactic center region.

Methanol Maser Emission from Galactic Center Sources with Excess 4.5 {\mu}m Emission