  It is shown how data on the cluster correlation function can be used in order
to reconstruct the density of the pregalactic density field on the cluster mass
scale. The method is applied to the data on the cluster correlation amplitude
-- richness dependence. The spectrum of the recovered density field has the
same shape as the density field derived from data on the galaxy correlation
function which is measured as function of linear scales. Matching the two
amplitudes relates the mass to the comoving scale it contains and thereby leads
to a direct determination of $\Omega$. The resultant density parameter turns
out to be $\Omega$=0.25.
