  We study the clustering properties of the recently compiled SDSS cluster
catalog using the two point correlation function in redshift space. We divide
the total SDSS sample into two richness subsamples, roughly corresponding to
Abell $R\ge 0$ and APM clusters, respectively. If the two point correlations
are modeled as a power law, $\xi(r)=(r_{\circ}/r)^{\gamma}$, then the
best-fitting parameters for the two subsamples are
$r_{\circ}=20.7^{+4.0}_{-3.8} h^{-1}$ Mpc with $\gamma=1.6^{+0.4}_{-0.4}$ and
$r_{\circ}=9.7^{+1.2}_{-1.2}$ with $\gamma=2.0^{+0.7}_{-0.5} h^{-1}$ Mpc,
respectively. Our results are consistent with the dependence of cluster
richness to the cluster correlation length. Finally, comparing the SDSS cluster
correlation function with that predictions from three flat cosmological models
($\Omega_{\rm m}=0.3$) with dark energy (quintessence), we estimate the cluster
redshift space distortion parameter $\beta \simeq \Omega_{\rm
m}^{0.6}/b_{\circ}$ and the cluster bias at the present time. For the
$\Lambda$CDM case we find $\beta=0.2^{+0.029}_{-0.016}$, which is in agreement
with the results based on the large scale cluster motions.
