We present an observational study investigating the presence, or lack thereof, of correlations between molecular tracers and the dynamical states of a set of protoplanetary disks. The dynamical states were measured through high-resolution ALMA observations as part of the exoALMA Large Program sample. We contrast these dynamical states with the emission of carbon-bearing species such as methanol (CH3OH) and formaldehyde (H2CO). Our research introduces a novel approach to exploring the relationship between the chemical complexity and dynamical evolution of protoplanetary disks, integrating both numerical models and observational data. We usually interpret molecular observations by forward-modelling them with quasi-equilibrium chemistry. It would be important to understand if this assumption is correct when disks are significantly stirred. The analysis will shed light on how the chemical composition in planet-forming disks changes and how some stellar properties, such as stellar mass for example, can play a predominant role or if the dynamical evolution of the disk overrides the stellar influence on the disk chemistry. Such understanding will illustrate whether disks can have a different intrinsic composition based on their dynamical evolution/state, and whether these variations can have long-term implications for the chemical reservoirs available for planet formation.