  We consider the long-standing problem of predicting the hierarchical
clustering amplitudes $S_p$ in the strongly non-linear regime of gravitational
evolution. N-body results for the non-linear evolution of the bispectrum (the
Fourier transform of the three-point density correlation function) suggest a
physically motivated ansatz that yields the strongly non-linear behavior of the
skewness, $S_3$, starting from leading-order perturbation theory. When
generalized to higher-order ($p>3$) polyspectra or correlation functions, this
ansatz leads to a good description of non-linear amplitudes in the strongly
non-linear regime for both scale-free and cold dark matter models. Furthermore,
these results allow us to provide a general fitting formula for the non-linear
evolution of the bispectrum that interpolates between the weakly and strongly
non-linear regimes, analogous to previous expressions for the power spectrum.
