  While the influence of galaxy clusters on galaxy evolution is relatively
well-understood, the impact of the dynamical states of these clusters is less
clear. This paper series explores how the dynamical state of galaxy clusters
affects their galaxy populations' physical and morphological properties. The
primary aim of this first paper is to evaluate the dynamical state of 87
massive ($M_{500} \geq 1.5 \times 10^{14} M_{\odot}$) galaxy clusters at low
redshifts ($0.10 \leq z \leq 0.35$). This will allow us to have a
well-characterized sample for analyzing physical and morphological properties
in our next work. We employ six dynamical state proxies utilizing optical and
X-ray imaging data. Principal Component Analysis (PCA) is applied to integrate
these proxies effectively, allowing for robust classification of galaxy
clusters into relaxed, intermediate, and disturbed states based on their
dynamical characteristics. The methodology successfully segregates the galaxy
clusters into the three dynamical states. Examination of the galaxy
distributions in optical wavelengths and gas distributions in X-ray further
confirms the consistency of these classifications. The clusters' dynamical
states are statistically distinguishable, providing a clear categorization for
further analysis.
