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We present multi-wavelength, high spatial resolution imaging of the IRS 7region in the R Corona Australis molecular cloud. Our observations include 1.1mm continuum and HCO^+ J = $3 \to 2$ images from the SMA, ^{12}CO J = $3 \to 2$outflow maps from the DesertStar heterodyne array receiver on the HHT, 450$\mu$m and 850 $\mu$m continuum images from SCUBA, and archival Spitzer IRACand MIPS 24 \micron images. The accurate astrometry of the IRAC images allow usto identify IRS 7 with the cm source VLA 10W (IRS 7A) and the X-ray source X_W.The SMA 1.1 mm image reveals two compact continuum sources which are alsodistinguishable at 450 $\mu$m. SMA 1 coincides with X-ray source CXOUJ190156.4-365728 and VLA cm source 10E (IRS 7B) and is seen in the IRAC andMIPS images. SMA 2 has no infrared counterpart but coincides with cm source VLA9. Spectral energy distributions constructed from SMA, SCUBA and Spitzer datayield bolometric temperatures of 83 K for SMA 1 and $\leq$70 K for SMA 2. Thesetemperatures along with the submillimeter to total luminosity ratios indicatethat SMA 2 is a Class 0 protostar, while SMA 1 is a Class 0/Class Itransitional object (L=$17\pm6$ \Lsun). The ^{12}CO J = $3 \to 2$ outflow mapshows one major and possibly several smaller outflows centered on the IRS 7region, with masses and energetics consistent with previous work. We identifythe Class 0 source SMA 2/VLA 9 as the main driver of this outflow. The complexand clumpy spatial and velocity distribution of the HCO^+ J = $3 \to 2$emission is not consistent with either bulk rotation, or any known molecularoutflow activity.

High Spatial Resolution Observations of Two Young Protostars in the R Corona Australis Region