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Upcoming wide-field surveys are well-suited to studying the growth of galaxyclusters by tracing galaxy and gas accretion along cosmic filaments. We usehydrodynamic simulations of volumes surrounding 324 clusters from \textsc{TheThreeHundred} project to develop a framework for identifying and characterisingthese filamentary structures, and associating galaxies with them. We define3-dimensional reference filament networks reaching $5R_{200}$ based on theunderlying gas distribution and quantify their recovery using mock galaxysamples mimicking observations such as those of the WEAVE Wide-Field ClusterSurvey. Since massive galaxies trace filaments, they are best recovered bymass-weighting galaxies or imposing a bright limit (e.g. $>L^*$) on theirselection. We measure the transverse gas density profile of filaments, derive acharacteristic filament radius of $\simeq0.7$--$1~h^{-1}\rm{Mpc}$, and use thisto assign galaxies to filaments. For different filament extraction methods wefind that at $R>R_{200}$, $\sim15$--$20%$ of galaxies with $M_*>3 \times 10^9M_{\odot}$ are in filaments, increasing to $\sim60%$ for galaxies more massivethan the Milky-Way. The fraction of galaxies in filaments is independent ofcluster mass and dynamical state, and is a function of cluster-centricdistance, increasing from $\sim13$% at $5R_{200}$ to $\sim21$% at $1.5R_{200}$.As a bridge to the design of observational studies, we measure the purity andcompleteness of different filament galaxy selection strategies. Encouragingly,the overall 3-dimensional filament networks and $\sim67$% of the galaxiesassociated with them are recovered from 2-dimensional galaxy positions.

Mapping and characterisation of cosmic filaments in galaxy cluster outskirts: strategies and forecasts for observations from simulations