[en] X-ray flares have routinely been observed from the supermassive black hole at our Galactic center, Sagittarius A${}^{\star <!--\; ???\; -->}$ (Sgr A^⋆). The nature of these flares remains largely unclear, despite many theoretical models. In this paper, we study the statistical properties of the Sgr A^⋆ X-ray flares by fitting the count rate (CR) distribution and the structure function of the light curve with a Markov Chain Monte Carlo method. With the 3-million-second Chandra observations accumulated in the Sgr A^⋆ X-ray Visionary Project, we construct the theoretical light curves through Monte Carlo simulations. We find that the 2–8 keV X-ray light curve can be decomposed into a quiescent component with a constant CR of $6\times <!--\; ??\; -->{10}^{-<!--\; ???\; -->3}$ count s⁻¹ and a flare component with a power-law fluence distribution $dN/dE\propto <!--\; ???\; -->E^{-<!--\; ???\; -->{\mathrm{\alpha <!--\; ??\; -->}}_{\mathrm{E}}}$ with ${\mathrm{\alpha <!--\; ??\; -->}}_{\mathrm{E}}=1.65\pm <!--\; ??\; -->0.17$. The duration–fluence correlation can also be modeled as a power law $T\propto <!--\; ???\; -->E^{{\mathrm{\alpha <!--\; ??\; -->}}_{\mathrm{E}\mathrm{T}}}$ with ${\mathrm{\alpha <!--\; ??\; -->}}_{\mathrm{E}\mathrm{T}}<<!--\; <\; -->0.55$ (95% confidence). These statistical properties are consistent with the theoretical prediction of the self-organized criticality system with the spatial dimension S = 3. We suggest that the X-ray flares represent plasmoid ejections driven by magnetic reconnection (similar to solar flares) in the accretion flow onto the black hole.