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Classic inflation, the theory described in textbooks, is based on the idea that, beginning from typical initial conditions and assuming a simple inflaton potential with a minimum of fine-tuning, inflation can create exponentially large volumes of space that are generically homogeneous, isotropic and flat, with nearly scale-invariant spectra of density and gravitational wave fluctuations that are adiabatic, Gaussian and have generic predictable properties.
P. J. Steinhardt, in The Very Early Universe , edited by G. Gibbons, H. S., and S. Siklos (Cambridge University Press, 1983) pp. 251–66
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