  In the first few Myr the massive stars dynamically interact, produce runaways
and affect the initial binary population. Observing and interpreting the
dynamics of young massive clusters is key to our understanding of the star
formation process and predicting the outcome of stellar evolution. We have
studied NGC6611 in the Eagle Nebula (M16), a young massive cluster hosting 19 O
stars. We used Gaia EDR3 data to determine the membership, age, cluster
dynamics and the kinematics of the massive stars including runaways. The
membership analysis yields 137 members located at a mean distance of 1706 $\pm$
7 pc. The colour - absolute magnitude diagram reveals a blue and a red
population of pre-main-sequence stars, consistent with two distinct populations
of stars. In line with earlier studies, the youngest population has a mean
extinction $A_V$ = 3.6 $\pm$ 0.1 mag and an age = 1.3 $\pm$ 0.2 Myr, while the
older population of stars has a mean extinction $A_V$ = 2.0 $\pm$ 0.1 mag and
an age = 7.5 $\pm$ 0.4 Myr. The latter population is more spatially extended
than the younger generation of stars. We argue that most of the OB stars belong
to the younger population. We identify 8 runaways originating from the center
of NGC6611, consistent with the dynamical ejection scenario. We show that ~ 50%
of the O stars have velocities comparable to or greater than the escape
velocity. These O stars can be traced back to the center of NGC6611 with
kinematic ages ranging from 0 to 2 Myr. This suggests that dynamical
interactions played an important role in the early evolution of NGC6611, which
is surprising considering the low current stellar density. Comparing this to
simulations of young massive clusters, the required initial radius of 0.1-0.5
pc is not consistent with that of NGC6611. The O stars could have initially
formed in wide binaries and possibly harden through dynamical interactions.
