Unlike their counterparts in the distant past, present-day supermassive black holes (SMBHs) at galaxy centers are typically very faint, particularly in X-ray. This phenomenon is exemplified by the dimness of the SMBH at our Galactic center, Sgr A*, which has an X-ray luminosity of a few $10^{33} {\rm~erg~s^{-1}}$, or a factor of $\sim 10^{11}$ lower than the Eddington luminosity limit. Even this low X-ray luminosity was recently proposed to be unrelated to the accretion of ambient matter by the SMBH and instead to be largely due to emission from a putative cusp of stars at the Galactic center. Based on the 3~million second Chandra/ACIS-S data, taken recently as part of the Sgr A* X-ray Visionally Program, we rule out this proposed scenario. Instead, we find that the X-ray spectrum of Sgr A* can be well explained by the so-called adiabatic inflow-outflow solution (ADIOS) of a radiatively inefficient accretion flow (RIAF). In particular, the radial density profile of the flow, tightly constrained by the X-ray data, matches the exact prediction of the solution, indicating that almost all captured matter is ejected back into the surrounding medium. There is also X-ray spectral evidence for the ejected plasma to be substantially hotter than the initial captured matter of a typical temperature $\sim 10^7$ K. As a result, little is left for the flow to radiate on the way into the SMBH. But such inflow-outflow behavior of SMBHs can have strong impact on their environments.