  We identify and characterise a Milky Way-like realisation from the Auriga
simulations with two consecutive massive mergers $\sim2\,$Gyr apart at high
redshift, comparable to the reported Kraken and Gaia-Sausage-Enceladus. The
Kraken-like merger ($z=1.6$, $M_{\rm Tot} = 8\times10^{10}\,$M$_{\odot}$) is
gas-rich, deposits most of its mass in the inner $10\,$kpc, and is largely
isotropic. The Sausage-like merger ($z=1.14$, $M_{\rm Tot} =
1\times10^{11}\,$M$_{\odot}$) leaves a more extended mass distribution at
higher energies, and has a radially anisotropic distribution. For the higher
redshift merger, the stellar mass ratio of the satellite to host galaxy is 1:3.
As a result, the chemistry of the remnant is indistinguishable from
contemporaneous in-situ populations, making it challenging to identify this
component through chemical abundances. This naturally explains why all
abundance patterns attributed so far to Kraken are in fact fully consistent
with the metal-poor in-situ so-called Aurora population and thick disc.
However, our model makes a falsifiable prediction: if the Milky Way underwent a
gas-rich double merger at high redshift, then this should be imprinted on its
star formation history with bursts about $\sim2\,$Gyrs apart. This may offer
constraining power on the highest-redshift major mergers.
