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Recent kinematical constraints on the internal densities of the Milky Way'sdwarf satellites have revealed a discrepancy with the subhalo populations ofsimulated Galaxy-scale halos in the standard CDM model of hierarchicalstructure formation. This has been dubbed the "too big to fail" problem, withreference to the improbability of large and invisible companions existing inthe Galactic environment. In this paper, we argue that both the Milky Wayobservations and simulated subhalos are consistent with the predictions of thestandard model for structure formation. Specifically, we show that there issignificant variation in the properties of subhalos among distinct host halosof fixed mass and suggest that this can reasonably account for the deficit ofdense satellites in the Milky Way. We exploit well-tested analytic techniquesto predict the properties in a large sample of distinct host halos with avariety of masses spanning the range expected of the Galactic halo. Theanalytic model produces subhalo populations consistent with both Via Lactea IIand Aquarius, and our results suggest that natural variation in subhaloproperties suffices to explain the discrepancy between Milky Way satellitekinematics and these numerical simulations. At least ~10% of Milky Way-sizedhalos host subhalo populations for which there is no "too big to fail" problem,even when the host halo mass is as large as M_host = 10^12.2 h^-1 M_sun.Follow-up studies consisting of high-resolution simulations of a large numberof Milky Way-sized hosts are necessary to confirm our predictions. In theabsence of such efforts, the "too big to fail" problem does not appear to be asignificant challenge to the standard model of hierarchical formation.[abridged]

Bailing Out the Milky Way: Variation in the Properties of Massive Dwarfs Among Galaxy-Sized Systems