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A key to understanding the formation of the first galaxies is to quantify thecontent of the molecular gas as the fuel for star formation activity throughthe epoch of reionization. In this paper, we use the 158$\mu$m [CII]fine-structure emission line as a tracer of the molecular gas in theinterstellar medium (ISM) in a sample of $z=6.5-7.5$ galaxies recently unveiledby the Reionization Era Bright Line Emission Survey, REBELS, with the AtacamaLarge Millimeter/submillimeter Array. We find substantial amounts of moleculargas ($\sim10^{10.5}\ M_\odot$) comparable to those found in lower redshiftgalaxies for similar stellar masses ($\sim10^{10}\ M_\odot$). The REBELSgalaxies appear to follow the standard scaling relations of molecular gas tostellar mass ratio ($\mu_{\rm mol}$) and gas depletion timescale ($t_{\rmdep}$) with distance to the star-forming main-sequence expected fromextrapolations of $z\sim1-4$ observations. We find median values at $z\sim7$ of$\mu_{\rm mol}=2.6_{-1.4}^{4.1}$ and $t_{\rm dep}=0.5_{-0.14}^{+0.26}$ Gyr,indicating that the baryonic content of these galaxies is gas-phase dominatedand little evolution from $z\sim7$ to 4. Our measurements of the cosmic densityof molecular gas, log$(\rho_{\rm mol}/(M_\odot {\rmMpc}^{-3}))=6.34^{+0.34}_{-0.31}$, indicate a steady increase by an order ofmagnitude from $z\sim7$ to 4.

The ALMA Reionization Era Bright Emission Line Survey (REBELS): The molecular gas content of galaxies at z~7