  The first non-trivial cumulant correlator of the galaxy density field
$Q_{21}$ is examined from the point of view of biasing. It is shown that to
leading order it depends on two biasing parameters $b$, and $b_2$, and on
$q_{21}$, the underlying cumulant correlator of the mass. As the skewness $Q_3$
has analogous properties, the slope of the correlation function $-\gamma$,
$Q_3$, and $Q_{21}$ uniquely determine the bias parameter on a particular scale
to be $b = \gamma/6(Q_{21}-Q_3)$, when working in the context of gravitational
instability with Gaussian initial conditions. Thus on large scales, easily
accessible with the future Sloan Digital Sky Survey and the 2 Degree Field
Survey, it will be possible to extract $b$, and $b_2$ from simple counts in
cells measurements. Moreover, the higher order cumulants, $Q_N$, successively
determine the higher order biasing parameters. From these it is possible to
predict higher order cumulant correlators as well. Comparing the predictions
with the measurements will provide internal consistency checks on the validity
of the assumptions in the theory, most notably perturbation theory of the
growth of fluctuations by gravity and Gaussian initial conditions. Since the
method is insensitive to $\Omega$, it can be successfully combined with results
from velocity fields, which determine $\Omega^{0.6}/b$, to measure the total
density parameter in the universe.
