  By assembling the largest sample to date of X-ray emitting EW-type binaries
(EWXs), we carried out correlation analyses for the X-ray luminosity
log$L_{\textrm{X}}$, and X-ray activity level
log($L_{\textrm{X}}$/$L_{\textrm{bol}}$) versus the orbital period $P$ and
effective temperature $T_{\rm eff}$. We find strong $P$-log$L_{\textrm{X}}$ and
$P$-log($L_{\textrm{X}}$/$L_{\textrm{bol}}$) correlations for EWXs with $P$ <
0.44 days and we provide the linear parametrizations for these relations, on
the basis of which the orbital period can be treated as a good predictor for
log$L_{\textrm{X}}$ and log($L_{\textrm{X}}$/$L_{\textrm{bol}}$). The
aforementioned binary stellar parameters are all correlated with
log$L_{\textrm{X}}$, while only $T_{\rm eff}$ exhibits a strong correlation
with log($L_{\textrm{X}}$/$L_{\textrm{bol}}$). Then, EWXs with higher
temperature show lower X-ray activity level, which could indicate the thinning
of the convective area related to the magnetic dynamo mechanism. The total
X-ray luminosity of an EWX is essentially consistent with that of an X-ray
saturated main sequence star with the same mass as its primary, which may imply
that the primary star dominates the X-ray emission. The monotonically
decreasing $P$-log($L_{\textrm{X}}$/$L_{\textrm{bol}}$) relation and the short
orbital periods indicate that EWXs could all be in the X-ray saturated state,
and they may inherit the changing trend of the saturated X-ray luminosities
along with the mass shown by single stars. For EWXs, the orbital period, mass,
and effective temperature increase in concordance. We demonstrate that the
period $P=0.44$ days corresponds to the primary mass of $\sim1.1 \rm M_\odot$,
beyond which the saturated X-ray luminosity of single stars will not continue
to increase with mass. This explains the break in the positive
$P$-log$L_{\textrm{X}}$ relation for EWXs with $P>0.44$ days.
