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This paper is the first in a series in which we perform an extensivecomparison of various galaxy-based cluster mass estimation techniques thatutilise the positions, velocities and colours of galaxies. Our primary aim isto test the performance of these cluster mass estimation techniques on adiverse set of models that will increase in complexity. We begin by providingparticipating methods with data from a simple model that delivers idealisedclusters, enabling us to quantify the underlying scatter intrinsic to thesemass estimation techniques. The mock catalogue is based on a Halo OccupationDistribution (HOD) model that assumes spherical Navarro, Frenk and White (NFW)haloes truncated at R_200, with no substructure nor colour segregation, andwith isotropic, isothermal Maxwellian velocities. We find that, above 10^14M_solar, recovered cluster masses are correlated with the true underlyingcluster mass with an intrinsic scatter of typically a factor of two. Below10^14 M_solar, the scatter rises as the number of member galaxies drops andrapidly approaches an order of magnitude. We find that richness-based methodsdeliver the lowest scatter, but it is not clear whether such accuracy maysimply be the result of using an over-simplistic model to populate the galaxiesin their haloes. Even when given the true cluster membership, large scatter isobserved for the majority non-richness-based approaches, suggesting that massreconstruction with a low number of dynamical tracers is inherentlyproblematic.

Galaxy Cluster Mass Reconstruction Project: I. Methods and first results on galaxy-based techniques