  We compare dynamics and waveforms from binary neutron star coalescence as
computed by new long-term ($\sim 10 $ orbits) numerical relativity simulations
and by the tidal effective-one-body (EOB) model including analytical tidal
corrections up to second post-Newtonian order (2PN). The current analytical
knowledge encoded in the tidal EOB model is found to be sufficient to reproduce
the numerical data up to contact and within their uncertainties. Remarkably, no
calibration of any tidal EOB free parameters is required, beside those already
fitted to binary black holes data. The inclusion of 2PN tidal corrections
minimizes the differences with the numerical data, but it is not possible to
significantly distinguish them from the leading-order tidal contribution. The
presence of a relevant amplification of tidal effects is likely to be excluded,
although it can appear as a consequence of numerical inaccuracies. We conclude
that the tidally-completed effective-one-body model provides nowadays the most
advanced and accurate tool for modelling gravitational waveforms from binary
neutron star inspiral up to contact. This work also points out the importance
of extensive tests to assess the uncertainties of the numerical data, and the
potential need of new numerical strategies to perform accurate simulations.
