  We measure the two point correlation function (CF) of 1357 galaxy clusters
with a mass of $\log_{10}{M_{200}}\geq 13.6$~\hm~and at a redshift of $z \leq
0.125$. This work differs from previous analyses in that it utilizes a
spectroscopic cluster catalogue, $\mathtt{SDSS-GalWCat}$, to measure the CF and
detect the baryon acoustic oscillation (BAO) signal. Unlike previous studies
which use statistical techniques, we compute covariance errors directly by
generating a set of 1086 galaxy cluster lightcones from the GLAM $N$-body
simulation. Fitting the CF with a power-law model of the form $\xi(s) =
(s/s_0)^{-\gamma}$, we determine the best-fit correlation length and power-law
index at three mass thresholds. We find that the correlation length increases
with increasing the mass threshold while the power-law index is almost
constant. For $\log_{10}{M_{200}}\geq 13.6$~\hm, we find $s_0 =
14.54\pm0.87$~\h~and $\gamma=1.97\pm0.11$. We detect the BAO signal at $s =
100$~\h~with a significance of $1.60 \sigma$. Fitting the CF with a
$\Lambda$CDM model, we find $D_\mathrm{V}(z =
0.089)\mathrm{r}^{fid}_d/\mathrm{r}_d = 267.62 \pm 26$ \h, consistent with
Planck 2015 cosmology. We present a set of 108 high-fidelity simulated galaxy
cluster lightcones from the high-resolution \U~N-body simulation, employed for
methodological validation. We find $D_\mathrm{V}(z = 0.089)/r_d = 2.666 \pm
0.129$, indicating that our method does not introduce any bias in the parameter
estimation for this small sample of galaxy clusters.
