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Polarized synchrotron emission from the radio halos of diffuse intraclustermedium (ICM) in galaxy clusters are yet to be observed. To investigate theexpected polarization in the ICM, we use high resolution ($1$\,kpc)magnetohydrodynamic simulations of fluctuation dynamos, which producesintermittent magnetic field structures, for varying scales of turbulent driving($l_{\rm f}$) to generate synthetic observations of the polarized emission. Wefocus on how the inferred diffuse polarized emission for different $l_{\rm f}$is affected due to smoothing by a finite telescope resolution. The meanfractional polarization $\langle p\rangle$ vary as $\langle p \rangle \proptol_{\rm f}^{1/2}$ with $\langle p \rangle > 20\%$ for $l_{\rm f} \gtrsim60$\,kpc, at frequencies $\nu > 4\,{\rm GHz}$. Faraday depolarization at $\nu <3$\,GHz leads to deviation from this relation, and in combination with beamdepolarization, filamentary polarized structures are completely erased,reducing $\langle p \rangle$ to below 5\% level at $\nu \lesssim1$\,GHz.Smoothing on scales up to $30$\,kpc reduces $\langle p \rangle$ above $4$\,GHzby at most a factor of 2 compared to that expected at $1$\,kpc resolution ofthe simulations, especially for $l_{\rm f} \gtrsim 100$\,kpc, while at $\nu <3$\,GHz, $\langle p \rangle$ is reduced by a factor of more than 5 for $l_{\rmf} \gtrsim 100$\,kpc, and by more than 10 for $l_{\rm f} \lesssim 100$\,kpc.Our results suggest that observational estimates of, or constrain on, $\langlep \rangle$ at $\nu \gtrsim 4$\,GHz could be used as an indicator of theturbulent driving scale in the ICM.

Properties of Polarized Synchrotron Emission from Fluctuation Dynamo Action -- II. Effects of Turbulence Driving in the ICM and Beam Smoothing