The power spectrum P ( k ) \propto k ^ { n } with n = -2 is close to the shape of the measured galaxy spectrum on small scales .
Unfortunately this spectrum has proven rather difficult to simulate .
Further , 2-dimensional simulations have suggested a breakdown of self-similar scaling for spectra with n < -1 due to divergent contributions from the coupling of long wave modes .
This paper is the second ( numerical ) part of our investigation into nonlinear gravitational clustering of scale-free spectra , in particular to test the scaling of the n = -2 spectrum .

Using high-resolution N-body simulations we find that the n = -2 power spectrum displays self-similar scaling .
The phase shift of Fourier modes of the density show a dual scaling , self-similar scaling at early times and a scaling driven by the bulk velocity at late times .
The second scaling was shown analytically to be a kinematical effect which does not affect the growth of clustering .
Thus our analytical and N-body results verify that self-similarity in gravitational clustering holds for -3 < n < 1 .
The N-body spectrum is also compared with analytic fitting formulae , which are found to slightly underestimate the power in the nonlinear regime .
The asymptotic shape of the spectrum at high- k is a power law with the same slope as predicted by the stable clustering hypothesis .